Nuclear heating in neutron star crusts

Journal Article · Fri Nov 17 04:00:00 EST 2006 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.2402622· OSTI ID:20894986

Brown, Edward F ^[1]

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1. National Superconducting Cyclotron Laboratory, Michigan State University, Dept. Physics and Astronomy, Michigan State University (United States)

A fluid element deposited onto the surface of an accreting neutron star is compressed by continual accretion. Here we describe calculations of the nucleosynthetic evolution of an accreted element from deposition into the atmosphere down to neutron drip density. These calculations are coupled with a solution of the thermal structure in the neutron star crust. In particular, we include temperature-dependent continuum electron capture rates and realistic sources of heat loss by thermal neutrino emission from the crust and core. In contrast to previous calculations, electron captures to excited states and subsequent {gamma}-emission significantly reduces the local heat loss due to weak-interaction neutrinos. These reactions release a large amount of heat at densities < 1011g cm-3, which can raise the local temperature and reduce the critical mass needed for unstable ignition of 12C.

• OSTI ID: 20894986
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 870; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
CARBON 12
CRITICAL MASS
DEPOSITION
ELECTRON CAPTURE
EVOLUTION
EXCITED STATES
HEAT LOSSES
NEUTRINOS
NEUTRON STARS
NEUTRONS
NUCLEOSYNTHESIS
PHOTON EMISSION
TEMPERATURE DEPENDENCE
WEAK INTERACTIONS